Extragalactic foregrounds are mostly compact sources consisting chiefly of AGNs and SFGs. Similar to the diffuse foregrounds, the extragalactic radio galaxy populations themselves are of immense scientific interest. The low-frequency population of radio sources is not yet adequately constrained, especially at the faint flux density end. There have been many surveys that have tried to provide a consensus on the number counts, luminosity functions, and other properties [1]}, [2]}, [3]}. The recent results from the LOFAR Two-Meter Sky Survey (LoTSS) have also started to explore the counts at the 150 MHz low flux end(see [4]} and references therein). The current deepest 150 MHz source counts from three extragalactic deep fields - Lockman Hole, ELAIS-N1, and Boötes, obtained using the LoTSSS data [4]} is shown in Figure REF . They are overlaid with counts from other surveys- Boötes at 150 MHz using LOFAR [6]} and GMRT observations of the ELAIS-N1 at 400 MHz [7]} and Lockman Hole at 325 MHz [8]}, [9]}. The AGNs dominate the flux densities \(\ge \) 1 mJy while SFGs dominate at the sub-mJy level. This is evident from the signature flattening of the counts at sub-mJy flux density levels. In addition to source counts, it is also essential to understand their spatial distribution (i.e., clustering). Ignoring clustering may result in underestimating the foreground power, leading to confusion in detecting the cosmological signal. It has been shown by [10]} that spatial clustering of extragalactic sources dominates the fluctuations for angular scales \(\theta \gtrsim 1^{\prime }\)  at 150 MHz (for flux density \(\gtrsim \) 0.1 mJy). Radio spectra of sources also need to be studied and modeled well since any deviation from the predicted smooth nature will make their removal challenging. Thus, a detailed study of the compact extragalactic sources in terms of the spatial, flux, and frequency characteristics will be required for EoR data sets.
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